J/AJ/156/276ivo://CDS.VizieR/J/AJ/156/276doi:10.26093/cds/vizier.51560276CDSDanielski C.Baudino J.-L.Lagage P.-O.Boccaletti A.Gastaud R.,Coulais A.Bezard B.2019-05-10T08:46:47Z2019-05-09T07:34:33ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frastronomical-modelsexoplanetsThe Mid-Infrared instrument (MIRI) on board the James Webb Space Telescope will perform the first ever characterization of young giant exoplanets observed by direct imaging in the 5-28 {mu}m spectral range. This wavelength range is key for both determining the bolometric luminosity of the cool known exoplanets and for accessing the strongest ammonia bands. In conjunction with shorter wavelength observations, MIRI will enable a more accurate characterization of the exoplanetary atmospheric properties. Here we consider a subsample of the currently known exoplanets detected by direct imaging, and we discuss their detectability with MIRI, either using the coronagraphic or the spectroscopic modes. By using the Exo-REM atmosphere model, we calculate the mid-infrared emission spectra of 14 exoplanets, and we simulate MIRI coronagraphic or spectroscopic observations. Specifically, we analyze four coronagraphic observational setups, which depend on (i) the target-star and reference-star offset (0, 3, 14 mas), (ii) the wavefront-error (130, 204 nm root mean square), and (iii) the telescope jitter amplitude (1.6, 7 mas). We then determine the signal-to-noise and integration time values for the coronagraphic targets whose planet-to-star contrasts range from 3.9 to 10.1 mag. We conclude that all the MIRI targets should be observable with different degrees of difficulty, which depends on the final in-flight instrument performances. Furthermore, we test for detection of ammonia in the atmosphere of the coolest targets. Finally, we present the case of HR 8799 b to discuss what MIRI observations can bring to the knowledge of a planetary atmosphere, either alone or in combination with shorter wavelength observations.2018AJ....156..276Dhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/AJ/156/276CatalogResearchIsServedByTAP VizieR generic servicerelated-toJ/ApJ/813/47 : Model atmospheres of irradiated exoplanets (Molliere+, 2015)https://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/AJ/156/276https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/AJ/156/276http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/AJ/156/276https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/AJ/156/276https://vizier.iucaa.in/viz-bin/votable?-source=J/AJ/156/276http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/AJ/156/276GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/AJ/156/276/catalogF1065C (table 10) , F1140C (table 11) and F1550C (table 12) 1{sigma} contrast curves as a function of the angular distance for observational cases k_A_, k_B_, k_C_, k_D_recnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintFilterFilter usedmeta.code;instr.filtercharDist[0.11/11] Angular distancearcsecpos.angDistancefloatkA[5e-09/9.9e-06] Contrast curve value for the k_A_ case (1)stat.fit.paramdoublekB[5.9e-08/0.00012] Contrast curve value for the k_B_ case (1)stat.fit.paramdoublekC[1.1e-07/0.00017] Contrast curve value for the k_C_ case (1)stat.fit.paramdoublekD[3.4e-07/0.00051] Contrast curve value for the k_D_ case (1)stat.fit.paramdouble